On the black hole mass–radio luminosity relation for flat-spectrum radio-loud quasars

Jarvis, Matt J.; McLure, R. J.

doi:10.1046/j.1365-8711.2002.05997.x

Cited by 56 publications

(53 citation statements)

References 31 publications

(52 reference statements)

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“…Their radio flux is Doppler boosted. Jarvis & McLure (2002) re-examined the relationship for the same sample as Oshlack et al (2002), who had found the relationship between radio luminosity and black hole mass to be independent. They pointed out that Doppler boosting may significantly influence the relationship and claimed that the correlation becomes significant after correcting for this effect.…”

Section: Discussionmentioning

confidence: 99%

“…Some authors have reported a correlation between radio Table 5 is available in electronic form at http://www.aanda.org luminosity and black hole mass (Franceschini et al 1998;Laor 2000;Lacy et al 2001;Jarvis & McLure 2002;Dunlop et al 2003;McLure & Jarvis 2004). However, other studies have not found this relationship (Ho 2002;Woo & Urry 2002;Oshlack et al 2002;Snellen et al 2003).…”

Section: Introductionmentioning

confidence: 99%

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The relationship between radio power at 22 and 43 GHz and black hole properties of AGN in elliptical galaxies

Park

Sohn

2013

A&A

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We investigate the relationship between radio power and properties related to active galactic nuclei (AGNs). Radio power at 1.4 or 5 GHz, which has been used in many studies, can be affected by synchrotron self-absorption and free-free absorption in a dense region. On the other hand, these absorption effects get smaller at higher frequencies. Thus, we performed simultaneous observations at 22 and 43 GHz using the Korean VLBI Network (KVN) radio telescope based on a sample of 305 AGN candidates residing in elliptical galaxies from the overlap between the Sloan Digital Sky Survey (SDSS) Data Release 7 and Faint Images of the Radio Sky at Twenty-Centimeters (FIRST). About 37% and 22% of the galaxies are detected at 22 and 43 GHz, respectively. Assuming no flux variability between the FIRST and KVN observations, spectral indices were derived from FIRST and KVN data and we found that over 70% of the detected galaxies have flat or inverted spectra, implying the presence of optically thick compact regions near the centres of the galaxies. Core radio power does not show a clear dependence on black hole mass at either low (1.4 GHz) or high (22 and 43 GHz) frequencies. However, we found that the luminosity of the [OIII] λ5007 emission line and the Eddington ratio correlate with radio power more closely at high frequencies than at low frequencies. This suggests that radio observation at high frequencies can be an appropriate tool for unveiling the innermost region. In addition, the luminosity of the [OIII] λ5007 emission line and the Eddington ratio can be used as a tracer of AGN activity. Our study suggests a causal connection between high frequency radio power and optical properties of AGNs.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The relationship between radio power at 22 and 43 GHz and black hole properties of AGN in elliptical galaxies

Park

Sohn

2013

A&A

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“…5 shows what the SKA, with a flux-density limit of S 200MHz > 100 nJy, will see in terms of radio-loud quasars (left) and radio-quiet quasars (right) as a fraction of the Eddington luminosity versus redshift for AGN with black-hole masses 10 6 M ⊙ < M bh < 10 9 M ⊙ . Given that powerful radio sources seem to require a supermassive black hole with mass > ∼ 10 8 M bh (Dunlop et al, 2003;Jarvis & McLure, 2002; then it is obvious from Fig. 5 that the SKA will easily detect all such sources.…”

Section: Supermassive Black Holes and Their Ac-mentioning

confidence: 99%

The accretion history of the universe with the SKA

Jarvis

Rawlings

2004

New Astronomy Reviews

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In this paper we investigate how the Square Kilometre Array (SKA) can aid in determining the evolutionary history of active galactic nuclei (AGN) from redshifts z = 0 → 6. Given the vast collecting area of the SKA, it will be sensitive to both 'radio-loud' AGN and the much more abundant 'radio-quiet' AGN, namely the radio-quiet quasars and their 'Type-II' counterparts, out to the highest redshifts. Not only will the SKA detect these sources but it will also often be able to measure their redshifts via the Hydrogen 21 cm line in emission and/or absorption. We construct a complete radio luminosity function (RLF) for AGN, combining the most recent determinations for powerful radio sources with an estimate of the RLF for radio-quiet objects using the hard X-ray luminosity function of Ueda et al. (2003), including both Type-I and Type-II AGN. We use this complete RLF to determine the optimal design of the SKA for investigating the accretion history of the Universe for which it is likely to be a uniquely powerful instrument.

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“…Specifically, studying the threshold for BH mass associated with the onset of significant radio activity is crucial for addressing basic questions about the physical process involved. According to the spectral analysis of homogeneous quasar samples, RLQs are associated to massive BHs with M BH 10 9 , while RQQs are linked to BHs with M BH 10 8 (Laor 2000;Jarvis & McLure 2002;Metcalf & Magliocchetti 2006). Other studies found that there is no such upper cutoff in the masses for RQQs and they stretch across the full range of BH masses (Oshlack et al 2002;Woo & Urry 2002;McLure & Jarvis 2004).…”

Section: Introductionmentioning

confidence: 99%

Probing the radio loud/quiet AGN dichotomy with quasar clustering

Retana-Montenegro

Röttgering

2017

A&A

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We investigate the clustering properties of 45441 radio-quiet quasars (RQQs) and 3493 radio-loud quasars (RLQs) drawn from a joint use of the Sloan Digital Sky Survey (SDSS) and Faint Images of the Radio Sky at 20 cm (FIRST) surveys in the range 0.3 < z < 2.3. This large spectroscopic quasar sample allow us to investigate the clustering signal dependence on radio-loudness and black hole (BH) virial mass. We find that RLQs are clustered more strongly than RQQs in all the redshift bins considered. We find a real-space correlation length of r 0 = 6.59 +0.33 −0.24 h −1 Mpc and r 0 = 10.95 +1.22 −1.58 h −1 Mpc for RQQs and RLQs, respectively, for the full redshift range. This implies that RLQs are found in more massive host haloes than RQQs in our samples, with mean host halo masses of ∼ 4.9 × 10 13 h −1 M and ∼ 1.9 × 10 12 h −1 M , respectively. Comparison with clustering studies of different radio source samples indicates that this mass scale of 1 × 10 13 h −1 M is characteristic for the bright radio-population, which corresponds to the typical mass of galaxy groups and galaxy clusters. The similarity we find in correlation lengths and host halo masses for RLQs, radio galaxies and flat-spectrum radio quasars agrees with orientation-driven unification models. Additionally, the clustering signal shows a dependence on black hole (BH) mass, with the quasars powered by the most massive BHs clustering more strongly than quasars having less massive BHs. We suggest that the current virial BH mass estimates may be a valid BH proxies for studying quasar clustering. We compare our results to a previous theoretical model that assumes that quasar activity is driven by cold accretion via mergers of gas-rich galaxies. While the model can explain the bias and halo masses for RQQs, it cannot reproduce the higher bias and host halo masses for RLQs. We argue that other BH properties such as BH spin, environment, magnetic field configuration, and accretion physics must be considered to fully understand the origin of radio-emission in quasars and its relation to the higher clustering.

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On the black hole mass–radio luminosity relation for flat-spectrum radio-loud quasars

Cited by 56 publications

References 31 publications

The relationship between radio power at 22 and 43 GHz and black hole properties of AGN in elliptical galaxies

The relationship between radio power at 22 and 43 GHz and black hole properties of AGN in elliptical galaxies

The accretion history of the universe with the SKA

Probing the radio loud/quiet AGN dichotomy with quasar clustering

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